The loss of ions from Venus through the plasma wake

  title={The loss of ions from Venus through the plasma wake},
  author={Stas Barabash and Andr{\'e}i Fedorov and J. Sauvaud and Rickard N. Lundin and Christopher T. Russell and Yoshifumi Futaana and T. L. Zhang and H. Andersson and Klas Brinkfeldt and Alexander Grigoriev and Mats Holmstr{\"o}m and Masatoshi Yamauchi and Kazushi Asamura and Wolfgang Baumjohann and Helmut Lammer and Andrew J. Coates and D. O. Kataria and D. R. Linder and Charles C. Curtis and Ke Chiang Hsieh and B. R. Sandel and Manuel Grande and Herbert Gunell and Hannu E. J. Koskinen and Esa Kallio and P{\"a}ivi Riihel{\"a} and T. S{\"a}les and Walter Schmidt and Janet Kozyra and Norbert Krupp and Markus Fr{\"a}nz and Joachim Woch and Janet G. Luhmann and Susan M. P. McKenna-Lawlor and Christian Xavier Mazelle and J. J. Thocaven and S. Orsini and R. Cerulli-Irelli and M. Mura and Michael T Milillo and Mario Maggi and Edmond C. Roelof and P C Brandt and Karoly Szego and John David Winningham and Rudy A. Frahm and J. R. Scherrer and James R. Sharber and Peter Wurz and Peter A. Bochsler},
Venus, unlike Earth, is an extremely dry planet although both began with similar masses, distances from the Sun, and presumably water inventories. The high deuterium-to-hydrogen ratio in the venusian atmosphere relative to Earth’s also indicates that the atmosphere has undergone significantly different evolution over the age of the Solar System. Present-day thermal escape is low for all atmospheric species. However, hydrogen can escape by means of collisions with hot atoms from ionospheric… 

Widely different characteristics of oxygen and hydrogen ion escape from Venus

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Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O + ions

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The nearly absence of water in the atmosphere of Venus is a major difference to the situation at Earth. The actual content of hydrogen in the exosphere is still an open issue, since no in situ



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[1] Space weather storms at the Earth are dominated by the magnetosphere's response to coronal mass ejections, or CMEs, whose disturbances propagate through the solar wind to 1 AU, and to a lesser

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In June 1979 the Pioneer Venus orbiter made its first series of passes through the distant solar wind wake of Venus at distances of 8–12 Rv behind the planet. During this period the plasma analyzer

Little or no solar wind enters Venus’ atmosphere at solar minimum

The bow shock under low solar activity conditions seems to be in the position that would be expected from a complete deflection by a magnetized ionosphere, therefore little solar wind enters the Venus ionosphere even at solar minimum.

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Pioneer Venus Orbiter plasma and magnetometer observations from the first nine tail seasons of crossings of the Venus wake are used to study ion pickup in the far wake of an unmagnetized object

Hot oxygen atoms in the upper atmosphere of Venus

The energy distribution of “hot” oxygen atoms in the upper atmosphere of Venus was calculated using two different numerical methods. The two different approaches were based on 1) 2-stream transport